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An attempt is made, probably for the first time, to understand the origin ofthe solar system in context with the evolution of the galaxy as a naturalconsequence of the birth of several generations of stellar clusters. The galaxyis numerically simulated to deduce the inventories of the short-lived nuclides,26Al, 36Cl, 41Ca, 53Mn and 60Fe, from the stellar nucleosynthetic contributionsof the various stellar clusters using an N-body simulation with updatedprescriptions of the astrophysical processes. The galaxy is evolved byconsidering the discreteness associated with the stellar clusters andindividual stars. We estimate the steady state abundance of the radionuclidesaround 4.56 billion years ago at the time of formation of the solar system.Further, we also estimate the present 26Al/27Al and 60Fe/56Fe of theinterstellar medium that match within a factor of two with the observedestimates. On contrary to the conventional galactic chemical evolution (GCE)model, the present adopted numerical approach provides a natural framework tounderstand the astrophysical environment related with the origin of the solarsystem. We deduce the nature of the two stellar clusters; the one that formedand evolved prior to the solar system formation, and the other within which thesolar system probably formed. The former could have contributed the short-livednuclides 129I and 53Mn, whereas, the supernova associated with the most massivestar in the latter contributed 26Al and 60Fe to the solar system. The analysiswas performed with the revised solar metallicity of 0.014.

The evolution of the galaxy and the birth of the solar system: The short-lived nuclides connection